The thermal structure of titan's upper atmosphere, I: Temperature profiles from Cassini INMS observations

D. Snowden, Roger Yelle, J. Cui, J. E. Wahlund, N. J T Edberg, K. Ågren

Research output: Contribution to journalArticle

42 Citations (Scopus)

Abstract

We derive vertical temperature profiles from Ion Neutral Mass Spectrometer (INMS) N2 density measurements from 32 Cassini passes. We find that the average temperature of Titan's thermosphere varies significantly from pass-to-pass between 112 and 175K. The temperatures from individual temperature profiles also varies considerably, with many passes exhibiting wave-like temperature perturbations and large temperature gradients. Wave-like temperature perturbations have wavelengths between 150 and 420km and amplitudes between 3% and 22% and vertical wave power spectra of the INMS data and HASI data have a slope between -2 and -3, which is consistent with vertically propagating atmospheric waves. The lack of a strong correlation between temperature and latitude, longitude, solar zenith angle, or local solar time indicates that the thermal structure of Titan's thermosphere is not primarily determined by the absorption of solar EUV flux. At N2 densities greater than 108cm-3, Titan's thermosphere is colder when Titan is observed in Saturn's magnetospheric lobes compared to Saturn's plasma sheet as proposed by Westlake et al. (Westlake, J.H. et al. [2011]. J. Geophys. Res. 116, A03318. http://dx.doi.org/10.1029/2010JA016251). This apparent correlation suggests that magnetospheric particle precipitation causes the temperature variability in Titan's thermosphere; however, at densities smaller than 108cm-3 the lobe passes are hotter than the plasma sheet passes and we find no correlation between the temperature of Titan's thermosphere and ionospheric signatures of enhanced particle precipitation, which suggests that the correlation is not indicative of a physical connection. The temperature of Titan's thermosphere also may have decreased by ~10K around mid-2007. Finally, we classify the vertical temperature profiles to show which passes are hot and cold and which passes have the largest temperature variations. In a companion paper (Part II), we estimate the strength of energy sources and sinks in Titan's thermosphere.

Original languageEnglish (US)
Pages (from-to)552-582
Number of pages31
JournalIcarus
Volume226
Issue number1
DOIs
StatePublished - Sep 2013

Fingerprint

Titan
upper atmosphere
thermal structure
temperature profile
temperature profiles
mass spectrometers
thermosphere
spectrometer
ion
ions
temperature
particle precipitation
Saturn
lobes
solar longitude
perturbation
plasma
wave power
solar flux
atmospheric wave

Keywords

  • Aeronomy
  • Atmospheres, structure
  • Titan, atmosphere

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

The thermal structure of titan's upper atmosphere, I : Temperature profiles from Cassini INMS observations. / Snowden, D.; Yelle, Roger; Cui, J.; Wahlund, J. E.; Edberg, N. J T; Ågren, K.

In: Icarus, Vol. 226, No. 1, 09.2013, p. 552-582.

Research output: Contribution to journalArticle

Snowden, D. ; Yelle, Roger ; Cui, J. ; Wahlund, J. E. ; Edberg, N. J T ; Ågren, K. / The thermal structure of titan's upper atmosphere, I : Temperature profiles from Cassini INMS observations. In: Icarus. 2013 ; Vol. 226, No. 1. pp. 552-582.
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